EDP Sciences
Free access
Issue
A&A
Volume 395, Number 2, November IV 2002
Page(s) 481 - 497
Section Stellar clusters and associations
DOI http://dx.doi.org/10.1051/0004-6361:20020790


A&A 395, 481-497 (2002)
DOI: 10.1051/0004-6361:20020790

The ages of the globular clusters M $\,$71 and 47 Tuc from Strömgren uvby photometry

Evidence for high ages
F. Grundahl1, P. B. Stetson2 and M. I. Andersen3

1  Institute of Physics and Astronomy, Aarhus University, Ny Munkegade, 8000 Aarhus C, Denmark
2  National Research Council, Herzberg Institute of Astrophysics, Dominion Astrophysical Observatory, 5071 W. Saanich Road, B.C., V9E 2E7, Canada
3  Division of Astronomy, University of Oulu, PO Box 3000, 90014 Oulun Yliopisto, Finland

(Received 19 February 2002 / Accepted 21 May 2002)

Abstract
New uvby CCD photometry for the fairly metal-rich globular clusters M $\,$71 (NGC 6838) and 47 Tuc (NGC 104) is presented. We derive the cluster distances using a sample of field subdwarfs with metallicities determined from uvby photometry and accurate parallaxes from the Hipparcos mission. The biases associated with the main-sequence fitting technique are discussed and only that due to metallicity is found to be significant, corresponding to a -0.05 $\,$mag change in distance modulus. Our main results are that: 1) The distance moduli of 47 $\,$Tuc and M $\,$71 are somewhat shorter than that derived by Reid (1998, AJ 115, 204). For M $\,$71 and 47 $\,$Tuc we find (metallicity corrected) $(m-M)_V\,=\,13.71\pm\,0.04\pm\,0.1$ and $(m-M)_V\,=\,13.33\pm\,0.04\pm\,0.1$, for adopted reddenings of $E(B-V)\,=\,0.28$ and $E(B-V)\,=\,0.04$ respectively (first errorbar denotes random errors and the second systematic errors). The main source of difference with Reid is the selection of subdwarfs with this study having more intrinsically faint field subdwarfs; 2) These values lead to ages of nearly 12 $\,$Gyr when using the isochrones of VandenBerg et al. ([CITE], ApJ, 532, 430); this estimate does not include the effects of He diffusion. 3) A differential comparison of the cluster colour-magnitude diagrams show that the age difference between the two is very small - less than one billion years. 4) The observed scatter in the c1 index (due to star-to-star nitrogen variations) among main-sequence stars does not allow us to use the [(v-y)0, c0] diagram for a distance-independent age determination.


Key words: globular clusters: individual: NGC 104, NGC 6838

Offprint request: F. Grundahl, fgj@phys.au.dk

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